J/A+A/595/A88 G345.45+1.50 13CO(3-2) clumps (Lopez-Calderon+, 2016)
G345.45+1.50: an expanding ring-like structure with massive star formation. Lopez-Calderon C., Bronfman L., Nyman L.-A., Garay G., de Gregorio-Monsalvo I., Bergman P. <Astron. Astrophys., 595, A88 (2016)> =2016A&A...595A..88L (SIMBAD/NED BibCode)
ADC_Keywords: Molecular clouds ; Carbon monoxide Keywords: ISM: clouds - stars: massive - stars: formation - dust, extinction - ISM: kinematics and dynamics - ISM: molecules Abstract: Ring-like structures in the interstellar medium (ISM) are commonly associated with high-mass stars. Kinematic studies of large structures in giant molecular clouds (GMCs) toward these ring-like structures may help us to understand how massive stars form. The origin and properties of the ring-like structure G345.45+1.50 is investigated through observations of the 13CO(3-2) line. The aim of the observations is to determine the kinematics in the region and to compare physical characteristics estimated from gas emission with those previously determined using dust continuum emission. This area in the sky is well suited for studies like this because the ring is located 1.5° above the Galactic plane at 1.8kpc from the Sun, thus molecular structures are rarely superposed on our line of sight, which minimizes confusion effects that might hinder identifying of individual molecular condensations. The 13CO(3-2) line was mapped toward the whole ring using the Atacama Pathfinder Experiment (APEX) telescope. The observations cover 17'x20' in the sky with a spatial resolution of 0.2pc and an rms of ∼1K at a spectral resolution of 0.1km/s. The ring is found to be expanding with a velocity of 1.0km/s, containing a total mass of 6.9x103M☉, which agrees well with that determined using 1.2mm dust continuum emission. An expansion timescale of ∼3x106yr and a total energy of ∼7x1046erg are estimated. The origin of the ring might have been a supernova explosion, since a 35.5cm source, J165920-400424, is located at the center of the ring without an infrared counterpart. The ring is fragmented, and 104 clumps were identified with diameters of between 0.3 and 1.6pc, masses of between 2.3 and 7.5x102M☉, and densities of between ∼102 and ∼104cm-3. At least 18% of the clumps are forming stars, as is shown in infrared images. Assuming that the clumps can be modeled as Bonnor-Ebert spheres, 13 clumps are collapsing, and the rest of them are in hydrostatic equilibrium with an external pressure with a median value of 4x104K/cm3. In the region, the molecular outflow IRAS 16562-3959 is identified, with a velocity range of 38.4km/s, total mass of 13M☉, and kinematic energy of 7x1045erg. Finally, five filamentary structures were found at the edge of the ring with an average size of 3pc, a width of 0.6pc, a mass of 2x102M☉, and a column density of 6x1021cm-2. Description: The 13CO(3-2) line observations were made at 330.588GHz using on-the-fly (OTF) observing mode with the APEX-2A heterodyne receiver mounted at the APEX telescope on October 17-19, 2005, May 28, June 24-26, and October 7-10, 2006. To estimate the gas temperature in the region, the 12CO(3-2) line was observed using ASTE toward 29 intensity peaks found in the 13CO(3-2) line map. Observations were made on August 27 2010. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tablef1.dat 62 104 Physical properties of the 13CO clumps
Byte-by-byte Description of file: tablef1.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq [1/104] Sequential number 5- 6 I2 h RAh Right ascension (
J2000) 8- 9 I2 min RAm Right ascension ( J2000) 11- 15 F5.2 s RAs Right ascension ( J2000) 17 A1 --- DE- Declination sign ( J2000) 18- 19 I2 deg DEd Declination ( J2000) 21- 22 I2 arcmin DEm Declination ( J2000) 24- 28 F5.2 arcsec DEs Declination ( J2000) 30- 32 F3.1 pc Dc Clump diameter 34- 39 E6.2 Msun Mc Clump mass 41- 43 F3.1 km/s DVc Clump 13CO line velocity width 45- 50 E6.2 cm-3 nc Clump 13CO density 52- 58 E7.2 cm-2 Nc Clump 13CO column density 60 A1 --- Type [ABC] Clump type (1) 62 A1 --- B-E [Y/N] indicates if clumps are candidates to be experimenting collapse (ξmax≥6.5)
Note (1): The clumps are classified into three types as follows: A = clumps have a counterpart seen in infrared and millimeter wavelengths B = clumps only have a counterpart in the 1.2mm continuum C = clumps are only seen in 13CO.
History: Prepared via OCR at CDS.
(End) Patricia Vannier [CDS] 15-Feb-2017
|The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line|